The preservation of mirror surface quality and figure are of paramount importance at the Navy Prototype Optical
Interferometer. There are on the order of 108 eight-inch optical flats mounted in the interferometer's optical train, 102 of
which are permanently mounted inside the 9000 cubic foot vacuum feed system. The flats are specified for manufacture
at λ/20 peak-to-valley surface variation (λ = 633 nm) over a 7.2 inch clear aperture. Silver coating with a dielectric
overcoat is subsequently applied to the reflecting surface. The objective when mounting the mirror is to preserve the
surface quality and figure of the coated flats as much as possible. Surface deflections occur due to pressure points
inherent in the mount. The mount consists of a modified commercially available tangent-arm gimbaled-type structure.
In order to minimize the mounting effects and allow for a wider thermal operational range, modifications were made to
the primary mirror cell in the following areas: edge support region, front face tabs, rear face loaders, and diameter. In
this paper we describe the detailed cell modifications, a finite element analysis (FEA) of the mounted flat, the free-standing
and as-mounted surface figure of a typical eight-inch diameter flat as measured with a phase-shifting
interferometer, the resulting mount-induced deflections, a comparison between the measured and FEA model, and
conclusions.
The Navy Prototype Optical Interferometer (NPOI) in Flagstaff, Arizona, makes use of separate smaller telescopes
spaced along a Y-array and used simultaneously to simulate an equivalent single large telescope. Each telescope is
mounted on a massive reinforced concrete pier tied to bedrock. The mass of the pier dampens most, but not all, of the
unwanted vibration in the required spectrum. The quality and resolution of a stellar image depends on minimizing
movement of the mirrors due to vibration. The main source of pier vibration is due to the soil-pier interaction.
Surrounding environmental and man-made vibration propagates through the soil as body and surface waves, and forces
the pier to move. In this paper, a novel concept based on a sleeve/air gap system to isolate the soil from the pier is used
to minimize the vibration input to the telescope. An example of the concept is presented with respect to the future
implementation of a 1.4-m diameter composite telescope at the Navy Prototype Optical Interferometer.
Engineering specifications for O-ring seal surfaces are well documented. However, when seal surfaces are located
on asymmetrically loaded vacuum end-plates, consideration must be given not only to surface finish and
flatness, but also to load-induced deflections. When deflections are significant, O-ring compression can relax
and potentially cause vacuum leaks. Large vacuum systems, such as the 9000 cubic foot system at the Navy
Prototype Optical Interferometer (NPOI), cannot afford costly vacuum leaks due to improper end-plate design.
The NPOI employs vacuum end-plates that serve both as structural members, and as vacuum system entrance
and exit ports for stellar light. These ports consist of vacuum components attached directly to the end-plate via
static O-ring sealing techniques. Optical geometry dictates off-center port locations, which create asymmetric
end-plate loading. This paper details the behavior of a 22 inch diameter, multi-port, end-plate for the NPOI Fast
Delay Line subsystem. In depth CAD modeling and finite element analysis techniques were used to determine
load-induced stress distributions and deflections in the end-plate. After several design iterations, an end-plate
design was substantiated that maintains vacuum seal integrity under loading, exhibits a conservative factor of
safety, and is readily manufacturable.
There are a total of one hundred seventy precision flat mirrors within the optical array at the Navy Prototype Optical
Interferometer (NPOI). During the build phase each mirror center is positioned in space relative to a primary fiducial.
Prior to nightly astronomy observations each mirror train, up to six trains containing ten mirrors each, are checked and
finely adjusted if necessary. The facilitation of diverse science programs and expanding capabilities at the NPOI require
reconfigurations of optical mounts. As part of this process, alignment of the reconfigured optical train is performed.
Similar tools and techniques are in use for each of these three processes. A light emitting diode (LED), mounted on a
motorized target arm is strategically attached to each mirror's mount for viewing the mirror's center point. A focusable
precision alignment telescope mounted in a precision v-block assembly is employed as the basic alignment tool. The
human eye is the detector. In this paper, we describe the current tools and techniques used at the NPOI to achieve the
requisite alignment tolerances and validations during the build, operations, and reconfiguration phases. We also discuss
the development of alignment tolerances, the deficiencies of the current tools and techniques, issues with digital imaging
and centroiding, and efforts to enhance, quantify, and validate the alignments.
The use of composite materials in the fabrication of optical telescope mirrors offers many advantages over conventional
methods, including lightweight, portability and the potential for lower manufacturing costs. In the construction of the
substrate for these mirrors, sandwich construction offers the advantage of even lower weight and higher stiffness.
Generally, an aluminum or Nomex honeycomb core is used in composite applications requiring sandwich construction.
However, the use of a composite core offers the potential for increased stiffness and strength, low thermal distortion
compatible with that of the facesheets, the absence of galvanic corrosion and the ability to readily modify the core
properties. In order to design, analyze and optimize these mirrors, knowledge of the mechanical properties of the core is
essential. In this paper, the mechanical properties of a composite triangular cell core (often referred to as isogrid) are
determined using finite element analysis of a representative unit cell. The core studied offers many advantages over
conventional cores including increased thermal and dimensional stability, as well as low weight. Results are provided
for the engineering elastic moduli of cores made of high stiffness composite material as a function of the ply layup and
cell size. Finally, in order to illustrate the use of these properties in a typical application, a 1.4-m diameter composite
mirror is analyzed using the finite element method, and the resulting stiffness and natural frequencies are presented.
Many aspects must be considered in the design of telescope enclosures. One critical aspect is the floor sensitivity to
movement. The floor moves due to floor-foundation interaction, floor-wall interaction, soil-floor interaction, and
internal enclosure loads. This paper presents the details of the design of an environmental enclosure floor having
minimum rotation due internal laboratory equipment loads, which can have a significant effect on the deformation of the
floor. Floor analysis is presented by finite element methods. An example of a floor design is presented in the context of
a future Navy Prototype Optical Interferometer (NPOI) environmental enclosure.
Reconfigurations of the original optical mounts are required to facilitate the expanding capabilities and diverse science
programs at the Navy Prototype Optical Interferometer. The mounts of current interest are tangent-arm gimbaled mounts
located in vacuum chambers, remotely controlled, and precisely aligned through a narrow range of motion. In order to
achieve the desired large changes in pathway reflections, the articulated range of the mount was increased from 4 to 45
degrees in elevation and from 4 to 90 degrees in azimuth. This increase was achieved on the elevation axis by fashioning
and attaching a worm gear device, and a direct-drive type mechanism was used on the azimuth axis. The original
alignment resolution and stability were preserved by retaining the high precision tangent-arm actuators. In this paper, we
present the design modifications that achieved the form, fit, and function required for remote-controlled reconfiguration
and alignment. The mechanical modifications, modes of operation, test results, and reconfigurations are described in
detail.
The portability of meter-class telescopes has been limited by the weight of the mirror, tube assembly and the mount required to provide pointing and tracking. The novel lightweight carbon fiber reinforced polymer telescopes being developed for array population at the Naval Prototype Optical Interferometer are orders of magnitude lighter than traditional telescopes. When combined with a lightweight carbon fiber mount, these telescopes will be easily transportable from one telescope station to another to change the interferometer baseline. The mount for a lightweight telescope is currently under development at Composite Mirror Applications, Inc. This paper reports on the design constraints of the mount, the scalability to larger aperture telescopes and the integration of sensors to measure the performance characteristics of this system during operation.
We have developed an approach for systematically investigating the optical throughput performance of the different segments of a Michelson stellar interferometer, and applied it to the characterization of the Navy Prototype Optical Interferometer (NPOI). We report the results of the first phase of throughput measurements on NPOI, as well as some of the lessons learned.
Since the current generation of ground-based optical interferometers all suffers from varying degree of throughput degradation while the dominant causes for throughput loss are expected to vary for each individual instrument, the methodologies and approaches developed here could be of general use for the quantitative characterization of the throughput performance of the different optical interferometers, a prerequisite for its ultimate improvement.
At the Navy Prototype Optical Interferometer (NPOI) we have developed a two-stage method for preparation and installation of the optical feed relay stations (elevators). This method reduces contamination, increases consistency, and allows greater management in testing and upgrades. In stage one, we prepare a pre-alignment facility in a laboratory. Using this facility we accurately position the feed stations, internal optics and detector optics relative to the NPOI array line-of-sight. The feed station is cleaned, assembled, internally aligned, tested and placed in its vacuum canister. It is stored under vacuum until transported to the array. In stage two, we align the station on the array by global five-axis adjustments of the vacuum canister. No further independent internal alignments are necessary. The canister is continuously under vacuum during global alignments. We describe the methodology and techniques for installing the optical feed stations.
At the Navy Prototype Optical Interferometer (NPOI), during stellar fringe acquisition and tracking, optical stations along the NPOI vacuum line array remain in passive mode. Optical drift amplitude and rate must remain below certain limits lest stellar acquisition and fringe tracking become unachievable. Subsequent to each observation, relay mirrors are reconfigured within the long delay line stations to provide appropriate constant delays. The placement of these mirrors must be reliable and repeatable within certain tolerances. We describe the results of drift tests conducted on the current long delay line stations.
The reflectivity of mirror surfaces is a critical aspect of telescope performance. This is especially true of large adaptive optics systems and interferometers where twenty or more reflective surfaces may be encountered prior to reaching the final detector. The ability to accurately measure the reflectivity of mirrors in-situ allows not only for the determination of system throughput, but also helps to determine when optical elements need cleaning or recoating. We compare the performance of three commercially available, hand-held reflectometers by measuring calibrated reference surfaces of varying reflectivity and scatter characteristics. The reference surfaces are precisely calibrated for absolute reflectivity against NIST traceable standards using a state-of-the-art laboratory reflectometer. Through analysis of the reflectometer measurements of the precisely calibrated surfaces, we determine the relative ability of each reflectometer to measure reflectivity and differentiate scattered light from specular reflection.
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